Three-body calculations of triple-alpha reaction

TL;DR

This paper presents a modified Faddeev three-body formalism to calculate the triple-alpha reaction rate, addressing discrepancies among previous methods and providing new insights into stellar nucleosynthesis at low temperatures.

Contribution

It introduces a modified Faddeev approach that accounts for Coulomb effects in three-body calculations of the triple-alpha process, offering a different reaction rate estimate.

Findings

Reaction rate is about 10 times larger than NACRE at 10^7 K.

Reaction rate is significantly smaller than recent three-body calculations.

Discusses reasons for differences in reaction rate estimates.

Abstract

Recently, the triple-\alpha (3\alpha) process, by which three 4He nuclei are fused into a 12C nucleus in stars, was studied by different methods in solving the quantum mechanical three-body problem. Their results of the thermonuclear reaction rate for the process differ by several orders at low stellar temperatures of 10^7 - 10^8 K. In this paper, we will present calculations of the 3\alpha process by a modified Faddeev three-body formalism in which the long-range effects of Coulomb interactions are accommodated. The reaction rate of the process is calculated via an inverse process, three-alpha (3-\alpha) photodisintegration of a 12C nucleus. Calculated reaction rate is about 10 times larger than that of the Nuclear Astrophysics Compilation of Reaction Rates (NACRE) at 10^7 K, and is remarkably smaller than the results of the recent three-body calculations. We will discuss a possible reason of the difference.